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Title:
On the nature of the extragalactic number counts in the K-band
Authors:
Barro, G.; Gallego, J.; Pérez-González, P. G.; Eliche-Moral, C.; Balcells, M.; Villar, V.; Cardiel, N.; Cristobal-Hornillos, D.; Gil de Paz, A.; Guzmán, R.; Pelló, R.; Prieto, M.; Zamorano, J.
Affiliation:
AA(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain ), AB(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain), AC(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain), AD(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain), AE(Instituto de Astrofísica de Canarias, vía Lactea, 38200 La Laguna, Canary Islands, Spain), AF(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain), AG(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain), AH(Instituto de Astrofísica de Andalucía, 18080 Granada, Spain), AI(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain), AJ(Department of Astronomy, 477 Bryant Space Center, University of Florida, Gainesville, FL, USA), AK(Laboratoire d'Astrophysique de Toulouse-Tarbes, CNRS, Université de Toulouse, 14 Avenue Edouard Belin, 31400 Toulouse, France), AL(Instituto de Astrofísica de Canarias, vía Lactea, 38200 La Laguna, Canary Islands, Spain), AM(Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain)
Publication:
Astronomy and Astrophysics, Volume 494, Issue 1, 2009, pp.63-79 (A&A Homepage)
Publication Date:
01/2009
Origin:
EDP Sciences
Keywords:
galaxies: evolution, galaxies: high-redshift, infrared: galaxies
DOI:
10.1051/0004-6361:200810633
Bibliographic Code:
2009A&A...494...63B

Abstract

Context: The galaxy number counts has been traditionally used to test models of galaxy evolution. However, the origin of significant differences in the shape of number counts at different wavelengths is still unclear. By relating the most remarkable features in the number counts with the underlying galaxy population it is possible to introduce further constraints on galaxy evolution.
Aims: We aim to investigate the causes of the different shape of the K-band number counts when compared to other bands, analyzing in detail the presence of a change in the slope around K ˜ 17.5.
Methods: We present a near-infrared imaging survey, conducted at the 3.5 m telescope of the Calar Alto Spanish-German Astronomical Center (CAHA), covering two separated fields centered on the HFDN and the Groth field, with a total combined area of 0.27 deg2 to a depth of K ˜ 19 (3σ, Vega). By combining our data with public deep K-band images in the CDFS (GOODS/ISAAC) and high quality imaging in multiple bands, we extract K-selected catalogs characterized with highly reliable photometric redshift estimates. We derive redshift binned number counts, comparing the results in our three fields to sample the effects of cosmic variance. We derive luminosity functions from the observed K-band in the redshift range [0.25-1.25], that are combined with data from the references in multiple bands and redshifts, to build up the K-band number count distribution.
Results: The overall shape of the number counts can be grouped into three regimes: the classic Euclidean slope regime (d log N/dm ˜ 0.6) at bright magnitudes; a transition regime at intermediate magnitudes, dominated by Mast galaxies at the redshift that maximizes the product φast{{dV_c}/{dΩ}}; and an α dominated regime at faint magnitudes, where the slope asymptotically approaches -0.4(α+1) controlled by post-Mast galaxies. The slope of the K-band number counts presents an averaged decrement of 50% in the range 15.5 < K < 18.5 (dlog N/dm˜0.6-0.30). The rate of change in the slope is highly sensitive to cosmic variance effects. The decreasing trend is the consequence of a prominent decrease of the characteristic density φastK,obs ( 60% from z=0.5 to z=1.5) and an almost flat evolution of MastK,obs (1σ compatible with MastK,obs=-22.89 ± 0.25 in the same redshift range).
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